Hostname: page-component-586b7cd67f-gb8f7 Total loading time: 0 Render date: 2024-11-23T02:30:12.589Z Has data issue: false hasContentIssue false

Aspects of Mass Loss and Angular Momentum Loss in Binaries Containing Cool Components

Published online by Cambridge University Press:  07 August 2017

Peter P. Eggleton*
Affiliation:
Institute of Astronomy Madingley Rd Cambridge CB3 0HA United Kingdom

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Cool stars show evidence of dynamo activity which is stronger with more rapid rotation. Tidal friction in a moderately close binary can be a cause of relatively rapid rotation, so that cool components in such binaries are presumably liable to stronger stellar winds than single cool stars. As a consequence, the binary can be subject to orbital angular momentum loss. Both the mass loss and the orbital angular momentum loss can be on a timescale comparable to nuclear evolution in a red subgiant, or even faster. RS CVn stars probably give the best possibility of measuring these processes, although some observational data are difficult to reconcile with simple theories.

Barium stars, and symbiotics, may both be affected by these processes. They must be the products of evolution of moderately wide binaries, as must such objects as cataclysmic variables. I attempt to define the ranges of zero-age parameters necessary to produce such varied objects. A simplistic model of the distribution of stars brighter than 6th magnitude (a ‘Theoretical Bright Star Catalogue’) suggests that for every three Ba stars with a measurable orbit, there should be one main sequence ‘Ba star’.

Type
Invited Papers
Copyright
Copyright © Kluwer 1992 

References

Boffin, H.M.J. and Jorissen, A. (1988) Astron. Astrophys. 205, 155 Google Scholar
Dominy, J.F. and Lambert, D.L. (1983) Astrophys. J. 270, 180 CrossRefGoogle Scholar
Eggleton, P.P., Fitchett, M.J. and Tout, C.A. (1990) Astrophys. J. 347, 998 CrossRefGoogle Scholar
Eggleton, P.P. and Tout, C.A. (1989) in IAU Coll 107, Algols, ed. Batten, A.H., p 165 Google Scholar
Griffin, R.F. (1985) in Interacting Binaries, ed. Eggleton, P.P. and Pringle, J.E. Reidel: Dordrecht p 1 Google Scholar
Hall, D.S. (1990) in Active Close Binaries, ed. İbanoglu, C., p 95 Google Scholar
Heintz, W.D. (1991) Astron. J. 101, 1071 CrossRefGoogle Scholar
Hoffleit, D. (1983) The Bright Star Catalogue , 4th edition; New Haven: Yale University Observatory Google Scholar
İbanoglu, C. (1990) in Active Close Binaries, ed. İbanoglu, C., p 515 Google Scholar
Judge, P.G. and Stencel, R.E. (1991) Astrophys. J. 371, 357 CrossRefGoogle Scholar
, P.K. (1991) Astron. J. 101, 2229 Google Scholar
Luck, R.E. and Bond, H.E. (1982) Astrophys. J. 259, 792 Google Scholar
Miller, G.E. and Scalo, J.M. (1979) Astrophys. J. Suppl. 41, 513 CrossRefGoogle Scholar
Mullan, D.J., Sion, E.M., Bruhweiler, F.C. and Carpenter, K.G. (1989) Astrophys. J. 339, L33 CrossRefGoogle Scholar
Paczynski, B. and Sienkiewicz, R. (1972) Acta Astron. 22, 73 Google Scholar
Popper, D.M. (1980) Ann. Rev. Astr. Ap. 18,115 Google Scholar
Popper, D.M. (1988) Astron. J. 96, 1040 CrossRefGoogle Scholar
Reimers, D. (1975) Mem. Soc. Roy. Sci. Liège 6e Ser. 8, 369 Google Scholar
Tomkin, J., Lambert, D.L., Edvardsson, B., Gustafsson, B. and Nissen, P.E. (1989) Astron. Astrophys. 219, L15 Google Scholar
Tout, C.A. and Eggleton, P.P. (1988a) Mon. Not. Roy. Astro. Soc. 231, 823 CrossRefGoogle Scholar
Tout, C.A. and Eggleton, P.P. (1988b) Astrophys. J. 334, 357 CrossRefGoogle Scholar